Pr0211

Last updated
Pr0211
Observation data
Epoch J2000        Equinox J2000
Constellation Cancer
Right ascension 08h 42m 11.49887s [1]
Declination +19° 16′ 37.2375″ [1]
Apparent magnitude  (V)12.143 [2]
Characteristics
Evolutionary stage Main sequence
Spectral type K1V [2] or late G [3]
Apparent magnitude  (G)11.926±0.003 [1]
Apparent magnitude  (J)10.660±0.022 [2]
Apparent magnitude  (H)10.242±0.019 [2]
Apparent magnitude  (K)10.173±0.016 [2]
Astrometry
Radial velocity (Rv)35.37±0.42 [1]  km/s
Proper motion (μ)RA: -36.820  mas/yr [1]
Dec.: -12.384  mas/yr [1]
Parallax (π)5.4387 ± 0.0184  mas [1]
Distance 600 ± 2  ly
(183.9 ± 0.6  pc)
Details [4]
Mass 0.935±0.013  M☉
Radius 0.827±0.012  R☉
Surface gravity (log g)4.51±0.05  cgs
Temperature 5300±30  K
Metallicity [Fe/H]0.18±0.02  dex
Rotation 7.97 days [5]
Rotational velocity (v sin i)5.1±0.3 km/s
Age 578±12 or 790±30  Myr
Other designations
Pr0211, EPIC  211936827, TIC  175291727, 2MASS J08421149+1916373, NGC 2632 JC 278 [2]
Database references
SIMBAD data

Pr0211 (sometimes written Pr 0211, also 2MASS J08421149+1916373) is a Sun-like late G or early K-type main-sequence star in the Beehive Cluster, or Praesepe, located 600 light-years away in the constellation Cancer. It is rotationally variable and has a rotation period of 7.97 days, [5] with its spin axis at an inclination of 76°±11° to the plane of the sky. [4] Pr0211 hosts two known exoplanets, and was the first multi-planet system to be discovered in an open cluster. [3] [4]

Pr0211 forms a binary star system with a K-type main-sequence star known as NGC 2632 JC 280 or 2MASS J08421285+1916040. [6] [7] [8]

Planetary system

Pr0211 b is a gas giant exoplanet, specifically a hot Jupiter, orbiting around Pr0211. Pr0211 b along with Pr0201 b are notable for being the first exoplanets discovered in the Beehive Cluster. [9] [10] Pr0211 b and Pr0201 b were discovered in 2012 by Sam Quinn [9] [10] [3] and his colleagues while observing 53 stars in the Beehive Cluster using the 1.5 metres (4.9  ft ; 1.6  yd ) telescope at the University of Georgia in the United States. [9]

Pr0211 c is a gas giant exoplanet orbiting around Pr0211. [11] Pr0211 c was discovered in 2016 by Luca Malavolta [11] [4] and his colleagues while observing its host star with the HARPS-N spectrograph on the 3.6 metres (12  ft ; 3.9  yd ) Italian Telescopio Nazionale Galileo (TNG) in La Palma, and the Tillinghast Reflector Echelle Spectrograph (TRES) mounted at the 1.5 metres (4.9  ft ; 1.6  yd ) telescope at the University of Georgia in the United States.

The Pr0211 planetary system [4]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b≥1.88±0.03  MJ 0.03176±0.000152.14610±0.000030.011+0.012
−0.008		——
c≥7.79±0.33  MJ 5.5+3.0
−1.4		4850+4560
−1750		0.71±0.11——

Related Research Articles

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<span class="mw-page-title-main">2M1207</span> Brown dwarf in the constellation Centaurus

2M1207, 2M1207A or 2MASS J12073346–3932539 is a brown dwarf located in the constellation Centaurus; a companion object, 2M1207b, may be the first extrasolar planetary-mass companion to be directly imaged, and is the first discovered orbiting a brown dwarf.

HD 46375 is double star with an exoplanetary companion in the equatorial constellation of Monoceros. It presents as an 8th-magnitude star with an apparent visual magnitude of 7.91, which is too dim to be readily visible to the naked eye. The system is located at a distance of 96.5 light-years from the Sun based on parallax measurements, but is slowly drifting closer with a radial velocity of −1 km/s. The common proper motion stellar companion, designated HD 46375 B, has a linear projected separation of 346±13 AU.

<span class="mw-page-title-main">Iota Horologii</span> Star in the constellation Horologium

Iota Horologii, Latinized from ι Horologii, is a yellow-hued star approximately 56.5 light-years away in the Horologium constellation. The star is classified as a G0Vp yellow dwarf. It has a mass and radius larger than the Sun, and is about 50% more luminous.

<span class="mw-page-title-main">HD 189733</span> Binary star system in the constellation Vulpecula

HD 189733, also catalogued as V452 Vulpeculae, is a binary star system 64.5 light-years away in the constellation of Vulpecula. The primary star is suspected to be an orange dwarf star, while the secondary star is a red dwarf star. Given that this system has the same visual magnitude as HD 209458, it promises much for the study of close transiting extrasolar planets. The star can be found with binoculars 0.3 degrees east of the Dumbbell Nebula (M27).

35 Cancri is a star in the zodiac constellation of Cancer, located 630 light years from the Sun. It is a challenge to view with the naked eye even under good seeing conditions, having an apparent visual magnitude of +6.55. The star is moving further from the Earth with a heliocentric radial velocity of +35 km/s, and is a member of the Beehive Cluster.

40 Cancri is a binary star system in the zodiac constellation of Cancer, located about 614 light years from the Sun in the Beehive Cluster. It is a challenge to view with the naked eye, having an apparent visual magnitude of 6.61. The system is moving further from the Earth with a heliocentric radial velocity of 34 km/s.

42 Cancri is a single star in the northern zodiac constellation of Cancer. With an apparent visual magnitude of 6.83, it is dimmer than what is considered the normal lower limit for visibility with the naked eye. The star is located at a distance of approximately 616 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +35 km/s. 42 Cancri is a member of the Beehive Cluster.

<span class="mw-page-title-main">XO-1</span> Star in the constellation Corona Borealis

XO-1 is a magnitude 11 G-type main-sequence star located approximately 530 light-years away in the constellation Corona Borealis. XO-1 has a mass and radius similar to the Sun. In 2006 the extrasolar planet XO-1b was discovered orbiting XO-1 by the transit method using the XO Telescope.

NGC 2423-3 is a red giant star approximately 3,040 light-years away in the constellation of Puppis. The star is part of the NGC 2423 open cluster. The star has an apparent magnitude of 10 and an absolute magnitude of zero, with a mass of 2.4 times the Sun. In 2007, it was proposed that an exoplanet orbits the star, but this is now doubtful.

<span class="mw-page-title-main">HD 80606 b</span> Eccentric hot Jupiter in the constellation Ursa Major

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HD 143361 is a star in the southern constellation Norma. With an apparent visual magnitude of 9.20, this star is too dim to be seen with the naked eye. It is close enough to the Earth that its distance can be determined using parallax measurements, yielding a value of 224 light-years.

HD 145377 is a star in the southern constellation Scorpius. It has an apparent visual magnitude of 8.10 and can be viewed with a small telescope. The star is located at a distance of 175 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +11.6. The absolute magnitude of this star is 4.31, indicating it would be visible to the naked eye if it were at a distance of 10 parsecs.

Kepler-39 is an F-type main sequence star located in the constellation Cygnus. It is located about 3,560 light-years away. One known substellar companion orbits it, Kepler-39b.

Kepler-19 is a G7V star that is host to three known planets - Kepler-19b, Kepler-19c, and Kepler-19d. It is located about 720 light-years away in the constellation Lyra, five arcminutes northwest of the much more distant open cluster NGC 6791.

HD 220689 is a single star in the equatorial constellation of Aquarius. It is a challenge to view with the naked eye, having an apparent visual magnitude of +7.74, but is readily viewed with a pair of binoculars. The star is located at a distance of 153 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +12 km/s. A survey in 2015 has ruled out the existence of any additional stellar companions at projected distances from 26 to 305 astronomical units.

Pr0201 b is an exoplanet orbiting around the F-type main-sequence star Pr0201. Pr0201 b along with Pr0211 b are notable for being the first exoplanets discovered in the Beehive Cluster located in the constellation Cancer. Since Pr0201 b has a mass of about half of Jupiter and an orbital period of about 4 days, it is likely a hot Jupiter. Its host star, Pr0201, is rotationally variable and has a rotation period of 5.63 days.

HD 233731, or HAT-P-22, is a suspected multiple star system in the northern circumpolar constellation of Ursa Major. It is invisible to the naked eye, having an apparent visual magnitude of 9.732. This system is located at a distance of 267 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +13 km/s.

<span class="mw-page-title-main">Gliese 15 Ac</span> Subjovian planet orbiting Gliese 15 A

Gliese 15 Ac is an exoplanet orbiting the nearby red dwarf star Gliese 15 A, which is part of a binary star system located about 11.6 light-years from the Sun. The planet was first proposed in October 2017 using radial velocity data from the CARMENES spectrograph, combined with measurements from the HARPS and HIRES spectrographs, and its existence was confirmed in April 2018 using HARPS-N data. It has a minimum mass 36 times that of Earth and orbits at around 5.4 astronomical units with a period of 7,600 days, an orbit which may have been sculpted by interaction with the companion star, Gliese 15 B. As of 2020, Gliese 15 Ac is the longest-period sub-Jovian planet discovered by radial velocity.

References

  1. 1 2 3 4 5 6 7 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. 1 2 3 4 5 6 "Cl* NGC 2632 JC 278". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 9 December 2023.
  3. 1 2 3 Quinn, Samuel N.; White, Russel J.; Latham, David W.; Buchhave, Lars A.; Cantrell, Justin R.; Dahm, Scott E.; Fűrész, Gabor; Szentgyorgyi, Andrew H.; Geary, John C.; Torres, Guillermo; Bieryla, Allyson; Berlind, Perry; Calkins, Michael C.; Esquerdo, Gilbert A.; Stefanik, Robert P. (2012). "Two 'b's in the Beehive: The Discovery of the First Hot Jupiters in an Open Cluster". The Astrophysical Journal. 756 (2): L33. arXiv: 1207.0818 . Bibcode:2012ApJ...756L..33Q. doi:10.1088/2041-8205/756/2/L33. S2CID   118825401.
  4. 1 2 3 4 5 Malavolta, L.; et al. (2016), "The GAPS programme with HARPS-N at TNG. XI. Pr 0211 in M 44: the first multi-planet system in an open cluster", Astronomy & Astrophysics, 588: A118, arXiv: 1602.00009 , Bibcode:2016A&A...588A.118M, doi:10.1051/0004-6361/201527933, S2CID   119207951
  5. 1 2 Kovács, Géza; Hartman, Joel D.; Bakos, Gáspár Á.; Quinn, Samuel N.; Penev, Kaloyan; Latham, David W.; Bhatti, Waqas; Csubry, Zoltán; De Val-Borro, Miguel (2014). "Stellar rotational periods in the planet hosting open cluster Praesepe". Monthly Notices of the Royal Astronomical Society. 442 (3): 2081. arXiv: 1405.3728 . Bibcode:2014MNRAS.442.2081K. doi:10.1093/mnras/stu946.
  6. ↑ Mugrauer, M. (December 2019). "Search for stellar companions of exoplanet host stars by exploring the second ESA-Gaia data release". Monthly Notices of the Royal Astronomical Society . 490 (4): 5088–5102. Bibcode:2019MNRAS.490.5088M. doi: 10.1093/mnras/stz2673 .
  7. ↑ "Pr0211". NASA Exoplanet Archive . Retrieved 9 December 2023.
  8. ↑ "Cl* NGC 2632 JC 280". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 9 December 2023.
  9. 1 2 3 Fazekas, Andrew (2012-09-21). "New Planets Found in Star Cluster - Would Have Dazzling Nights". National Geographic News. NATIONAL GEOGRAPHIC. Archived from the original on September 23, 2012. Retrieved 2016-05-30.
  10. 1 2 "Planet Pr 0211 b". Extrasolar Planets Encyclopaedia . Retrieved 2016-04-18.
  11. 1 2 "Planet Pr 0211 c". Extrasolar Planets Encyclopaedia . Retrieved 2016-04-18.
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